The team:
JHeidt (LSW): Lead, coordination + everything
WSeifert (LSW): Co-lead, coordination + everything
SEsposito (Arcetri): Lead AO-team
GAgapito (Arcetri): AO-team
EPinna (Arcetri): AO-team
APuglisi (Arcetri): AO-team
IStilz (LSW): Acq. and alignment tool (remote)
PBuschkamp (MPE): MOS (remote)
HGemperlein (MPE): MOS (remote)
Detector-Team (MPIA): Detector (remote)
APramskiy (AIRUB): Software
DThompson (LBTO): Support obs, data reduction + analysis, anything else tbd
MEdwards (LBTO): Support obs, data reduction + analysis, anything else tbd

Times given refer to amount to finish the task excl. overhead

DAYTIME (Closed Dome) Tests . . . . . . . . . . . . .

Test Status Time Test Status Time
Internal flexure N30 camera Pending 4h Non-common path aberration Partly done 3d
Image quality N30 camera Open 1h NCPA wrt to seeing Partly done 3d
Spec. res. & grat. disp. G40 Open 2h Diff. flexure pyramid - LUCI2 Open 2.5d
Software functionality Open 3d AO correction and vibrations Partly done --
Alignment of system Done 5d Active flexure compensation Open 5h
System performance Open 3d      
NIGHTTIME (On Sky) Tests . . . . . . . . . . . . .

Test Status Time Test Status Time
Offset LUCI2 FP vs hotspot CCD 47 Open 3h Achievable Srehl Open 9h
Slope null compensation Open 18h LS acquisition and alignment procedures Open 5h
AO Pyramid stage transform Open 6h ADC performance Open 3h
Accuracy of offsets, jitter etc. Open 3h Spectroscopic image quality Open 3h
Image scale N30 camera Open -- Ghosts, scattered light Open 2h
Image distortion N30 camera Open -- Variability of PSF Open 6h
Photometric ZP N30 camera Open 2h Image movement due to flexure in AO mode Open 5h
Image quality N30 camera Open 6h Active flexure compensation Open 5h
Open : Data have not yet been taken
Partly done: Data partly taken, eg confirmation measurements still lacking
Pending: Data taken but not yet analysed
Done : Data taken and analysed, task completed

DAYTIME (Closed Dome) Tests . . . . numbers in brackets refer to commissioning plan version 2.4. . . . . .

  • Internal flexure N30 camera (7.3.1)
  • Image quality N30 camera (7.3.2)
  • Spectral Resolution and Grating Dispersion G40 with N30 camera (7.3.3)
  • Software functionality (7.3.4)
  • Alignment of system (7.3.5)
  • System performance (7.3.6)
  • Non-common path aberration (7.3.7)
  • 7.3.7 wrt to seeing (7.3.8)
  • Diff. flexure pyramid - LUCI2 (7.3.9)
  • AO correction and vibrations (7.3.10)
  • Active flexure compensation (7.3.11)

NIGHTTIME (On Sky) Tests . . . . . numbers in brackets refer to commissioning plan version 2.4.. . . . . .

  • Offset LUCI2 FP vs hotspot CCD 47 (7.4.1)
  • Slope null compensation test (7.4.2)
  • AO Pyramid stage transformation (7.4.3)
  • Accuracy of offsets, jitter, nodding (7.4.4)
  • Image scale N30 camera (7.4.5)
  • Image distortion N30 camera (7.4.6)
  • Photometric ZP N30-camera (7.4.7)
  • Image quality N30 camera (7.4.8)
  • Achievable Strehl (7.4.9)
  • Longslit acquisition and alignment procedures (7.4.10)
  • ADC Performance (7.4.11)
  • Spectroscopic image quality (7.4.12)
  • Ghosts, scattered Light (7.4.13)
  • Variability of PSF (7.4.14)
  • Image movement due to flexure in AO mode on sky (7.4.15)
  • Active flexure compensation (7.4.16)

On-telescope day-time (closed dome) calibrations:

*Scripts for closed-dome activites are placed in folder daytime_com at the LUCI machine*

Internal Flexure N30 camera, duration 4hrs

Item: Measurement of the internal flexure of the instrument
Responsible: WSeifert
Phase: Before AO Com#1 on sky
Procedure: Measurements of the internal flexure of the instrument for N30camera in imaging and spectroscopic mode.
Remarks: Input for flexure compensation. An initial set of data has been taken during the LBTB-run Dec 3-9 2014. Data set for verification still required.

Image Quality N30 camera, duration 1hr


Item: Point spread function (PSF, as a measure for image quality) over the field with N30 camera for all broad-band filters.
Responsible: WSeifert, JHeidt
Phase: Before AO Com#1 on sky
Procedure: Take images with Optic Sieve mask.
Remarks: Full check under operation during night is required.

Spectral Resolution and Grating Dispersion G40 with N30 camera, duration 2hrs


Item: Evaluation of dispersion and resolution via line width
Responsible: JHeidt
Phase: As early as possible
Procedure: Taking spectra with the grating G40 and the N30 camera using wavelength calibration lamps to determine spectral resolution.
Prerequisites: G40 installed


Software functionality, duration 3 days


Item: Check the AO SW functionalities and its interaction with the LUCI2 control SW
Responsible: APuglisi, LFini, APramskiy
Procedure: The SW commands used to operate LUCI2 in adaptive
mode should be tested to verify that they are properly executed. The
daytime tests should be done as much as possible with the telescope
simulating the observing mode. The procedure for each single command
test will be detailed between the AO SW and the LUCI2 SW
responsible. The LBTO TCS SW responsible might be required for
troubleshooting and/or for learning LUCI2's interaction with the AO.
Duration: Estimated duration for such tests is 3 days
including SW debugging. It can be reduced to 1 day if as much as possible
is been done before, but given the current time-line there seems to be no
opportunity to do so
Prerequisites: Both systems (LUCI2 and FLAO) installed at the telescope.

Alignment of on-axis WFS with LUCI2 dichroic, duration 1+4days


Item: Alignment of the on-axis WFS with LUCI dichroic.
Responsible: S. Esposito
Procedure:
Discussion with W. Seifert and J. Storm showed that mating
LUCI2 and AGW unit in the optical lab requires designing new
HW and using a new procedure. This has been seen as a major
risk and a new alignment procedure has been identified that
do not require mating the two units. This second procedure
still requires to have the two instruments in the optical lab.
1) To install a dummy LUCI window on the AGW unit. We have
the HW already developed in Arcetri to mount it. The HW was
developed during the solar tower test.
2) To put this dummy window in the proper orientation with
the laser tracker following measurement of the real window
on LUCI2 in the lab.
3) To do the auto-collimation of the WFS board by using our
standard procedure and the dummy LUCI window placed in
the correct position.
Our proposal is to use this new procedure. The expected
time is about 4 days as for the previous one. We will
require support from LBTO to provide the laser tracker
measurements during this period.
Duration: 2 x 0.5days for moving LUCI2+AGw down to the lab
and back, measurements take 4 days in the lab.
Prerequisites: LUCI2+AGw down in the lab

Measure system performance via retro-reflector and verify system calibrations, duration 3 days

Item: SR measurements using images taken with LUCI2.
Images are acquired in H band.
Responsible: AO-team
Procedure: The internal reference source of the W unit is
used as point source to and AdSec actuators are loaded with a proper time
history to simulate atmospheric turbulence. The loop is closed and the
gains optimized. The SR value in H band is measured and compared with
expected results from simulations.
See also: FLAO system commissioning report
Duration: 3 days including the system interaction matrix
calibration at different binnings.
Prerequisites: The system has to be aligned, data reduction
SW for SR computation available and validated, slope null vector for on
axis sources available if needed.
Remarks: SR measurements with no simulated turbulence
will be acquired to verify the maximum achievable SR with no disturbance.

Non-common path aberration, duration 3 days


Item: Identification of slope null vector for NCPA correction
Responsible: AO-team, LUCI-team
Procedure: The planned procedure is the same that has a
been used with IRTC to identify NCPA due to the transmission of the
IR light in the IRTC dichroic. The procedure consists to apply a certain
number to low order modes and identify for each of this modes the best
coefficients in terms of achieved SR. The final signal generated by
the full set of identified modes is saved as slope null vector.
Prerequisites: The system has to be aligned, function to save
LUCI2 images are available.
Remarks: The images acquisition procedure should be
tested to achieve the fastest possible frame rate. This will speed
up the tests where a frame rate of 10-30 Hz is required.
The LBTO AO group may use their own phase-diversity-approach to
determine the NCPA. Comparing both approaches would be very useful as cross
check for this important measurement. To be coordinated between the Arcetri
and the LBTO AO team

Check NCPA w.r.t. to seeing (Slope0-vector), duration 3 days

Item: Slope null vector behavior w.r.t. seeing.
Responsible: AO-team
Procedure: To be identified.
Prerequisites:Slope null vector for a given NCPA has been identified.
Remarks: The procedure to adjust the slope null vector as
a function of the seeing changes is currently under study using simulations.

Differential flexure between pyramid and LUCI2, duration 2.5 days

Item: Differential flexure between WFS and LUCI2.
Responsible: AO-team, LUCI-team
Procedure: We assume that the global differential flexure
between pyramid focal plan and LUCI detector plane can be measured for a
given LUCI camera. To do this we have to go trough the following steps.
The RR has to be installed for such a test.
1) Put the telescope at a given elevation.
2) Rotate the instrument rotator at a given position.
3) Close the loop on AO
4) Measure the spot position on LUCI detector.
5) Repeat the measurement (4) for a given set of instrument
rotator angles. The actual number of angles will depend on
the flexure amplitudes and required flexure correction accuracy.
Steps 2 to 5 are repeated for a different elevation angle. The
actual number of elevation angles will depend on the flexure
amplitude and required flexure correction accuracy. In all
measurements the spot is initially placed to the same reference pixel.
If the LUCI detector plan flexures w.r.t telescope focal plane
are known we can find the pyramid focal plane flexure w.r.t
telescope focal plane, if needed.
Duration: 2.5 days. May be shortened if we restrict ourselves
to eg one elevation, but needs to be done for a few at least once.

AO correction and vibrations


Item: AO correction and vibrations
Responsible: AO-team, LUCI-team
Procedure: This task should be done in parallel with the
estimate of the achievable performance in daytime. The tip tilt spectrum
should be analyzed to identify if any vibrations do affect the achieved
results. This can be done by using diagnostic data from the AO system
or fast readout (30/50 Hz) of a sub-array of the LUCI2 detector if possible.
Duration: In parallel with performance tests
Remarks: LUCI team availability to test different conditions
of the instrument especially considering cryo coolers.


Active flexure compensation, duration 5hrs


Item: Tests for active flexure compensation. Verification of procedure.
Responsible: LUCI-Team
Remarks: Novel, may require fine-tuning.


On-telescope night-time on-sky calibrations:

Offset LUCI2 FP vs hotspot CCD 47 - Verification, duration 3hrs


Item: Offset between LUCI2 focal plane and the CCD47 hot spot.
Responsible: AO-team
Phase: AO-Com#1
Procedure: An on‐axis star will be offset in
AO Closed loop to a preferred spot on the LUCI2 detector and the
offset values be "put into" the PCS configuration variables
to change the default pointing origin. Than the current Wunit stage
X,Y positions should be put into the AO System configuration
as the Wunit stage on‐axis position. The result is that a preset, if
the pointing model is accurate, should put the target star on or near
the correct position on LUCI2. Acquisition and Guiding by the
AGw should put the target star at the correct position. The AO reference
star should then be very close to landing on the peak of the pyramid
sensor. AO closed loop will move the Wunit stage so the reference star
light is on the peak of the pyramid and the position of the target
star on the LUCI2 array should at the preferred spot set above
in the first step.
Weather: No restrictions
Targets: Bright (rmag = 8-12) stars for on-axis WFS.
Specs: Source should be centered in x on the AO slit.


Slope null compensation test, duration 18hrs


Item: Verification that slope null compensation tested during daytime is
working in real turbulence conditions
Responsible: AO-team
Phase: AO-Com#1
Procedure: Done on stars with different mag (8, 12, 16) and with
on/off-axis configuration of the RS.
Weather: Thin cirrus, seeing < 1" on guider
Prerequisites: Preceding closed-dome tests must have successfully been executed.
Targets: WFS stars with rmags between 8 and 16 (18?). For offaxis WFS stars the "observed"
star should have always comparable brightness.
Specs: Slope nulll compensation should be comparable to the one in closed-dome
Remarks: To be done at beginning of nighttime AO commissioning.
Optimize for highest SR applications but at lower sensitivity and dynamical range
vs. highest sensitivity when science depends not critically on SR.


AO Pyramid stage transformation, duration 2 * 3hrs


Item: Determine AO Pyramid stage transformation.
Responsible: LBTO
Phase: AO-Com#1 (ideally before)
Procedure: Take images of astrometric stars spread across the
patrol field at various PA.
Weather: No restrictions
Prerequisites: AO loop can be closed.
Targets: Sufficiently densely sampled field
(~20-30 stars in AO patrol field with rmag $>$ 15.5)
with good astrometry (eg. globular cluster imaged by HST).
Specs: Repeatability ~ 6mas (~ 4microns) rms
Remarks: First set of data taken to derive AO Pyramid stage
transformation, second set of data for verification. May require a second iteration.

Accuracy of offsets, jitter, nodding, duration 3hrs

Item: Accuracy of (large) offsets, jitter and nodding - critical for narrow slits
Responsible: LUCI-Team
Phase: AO-Com#1
Procedure: Imaging of sources by nodding, jittering and large offsets, tests ADI
Weather: Thin cirrus, seeing < 1.2"
Targets: No restrictions
Prerequisites: AO Pyramid stage transform in place.
Specs: Accuracy same as derived for AO pyramid stage transformation.
Remarks: Could be used for PR-purposes

Image Scale for N30 camera

Item: Image scale for N30 camera
Responsible: LUCI-Team
Phase: First run, to be regularly checked during all commissioning phases
Procedure: Imaging of stars with precisely known angular distances in
N30 mode. Take into account scale variation caused by the telescope, if measurable
Weather: Thin cirrus, seeing < 1.2"
Targets: & Sufficiently densely sampled field with good astrometry (eg. globular cluster imaged by HST)
Specs: & Identical to measurements with Optic Sieve
Remarks: Can be done together with image quality measurements. Data from other tests can be used.

Image Distortion N30 camera

Item: Astrometric calibration over the field, as a function of filter
setting for the N30 camera
Responsible: LUCI-Team
Phase: First-run, some time to be re-checked in later commissioning phases
Procedure: ake image of astronomic star cluster and derive distortion
Weather: Thin cirrus, seeing < 1.2"
Targets: Sufficiently densely sampled field with good astrometry (eg. globular cluster imaged by HST)
Specs: Identical to measurements with Optic Sieve
Remarks: Can be done together with image quality measurements.

Photometric ZP N30-camera, duration 2hrs

Item: Determine photometric ZP for all LUCI2-filters
Responsible: LUCI-Team
Phase: Whenever observing conditions allow
Procedure: Imaging with N30 camera
Weather : Photometric, seeing < 1.2"
Targets: Photometric standards.
Specs: Scatter (residuals AM vs ZP) below 0.2mag
Remarks: Can be done open loop. 2hrs given above a for BB-filters and
1-2 nB/mB-filters. If all filters should be measured nighttime required amounts to at least 6hrs.

Image Quality under diffraction-limited observing conditions, duration 6 hrs

Item: Determine Strehl ratio and FWHM on corrected images
over the field with N30 camera for all BB and some MB/NB-filters.
Responsible: LUCI-Team
Phase: All phases
Procedure: Imaging of stars distributed over the FOV covering the whole
instrument wavelength range
Weather: Thin cirrus, excellent/OK/poor seeing (test each once)
Targets: Globular cluster, potentially Nb-filters for brighter stars
Specs: N/A
Remarks: Can also be used to optimize best focus
position for the Guide/WFSC probe stage (off-axis WFSC can collect images for analysis).

Achievable Strehl, duration 9 hrs

Item: Determine Strehl as function of mag RS, distance RS,
input seeing elevation in the one BB (H)-filter. Provides ``grid'' for users manual.
Responsible: LUCI-Team, AO_Team
Phase: All phases
Procedure: Imaging with N30 camera using RS's with varying mag (8-16 in
steps of 2mag), distance from center and elevation
Weather: Thin cirrus, excellent/OK/poor seeing (test each once), excellent seeing more detailed
Targets: Globular cluster, potentially Nb-filters for brighter stars
Specs: N/A, comparison/difference to IRTC obs.
Remarks: Results are partly known from AO-com/Pisces/IRTC-observations.
Observations from image quality measurements can also be used. If the test is to be done
as outlined above this will result in a huge amount of observing time. It is probably be
better to take Fig. 3 from Simones SPIE paper with the results of the FLAO #1-com with
IRTC as reference and to coarsely sample the parameter space. The outcome could eg an
offset/shift wrt to FLAO #1-com results. Particularly interesting is the magnitude
range 12-18 where Fig. 3 is lacking reliable ambient seeing values.

Acquisition and Alignment Procedures (Software), duration 5hrs

Item: Acquisition and alignment in longslit mode (spectroscopy)
Responsible: LUCI-Team
Phase: AO-Com #1 if possible, but can also be done later
Procedure: Check software accuracy and reliability of acquisition and alignment
Weather: Thin cirrus (photometric if check for throughput), seeing < 1.2"
Targets: Tellurics
Specs: Accuracy 1/10th of slit
Remarks: No grating for spectroscopy available during AO-Com #1

ADC Performance, duration 3hrs

Item: Investigate proper compensation of atmospheric dispersion
by ADC in J and H filters
Procedure: Observe stars at large zenith distances and check for dispersion
Weather: Clear
Prerequisites: star; good image quality
Targets: Tellurics
Specs: Resume perfect lambda-performance

Spectroscopic Image Quality, duration 3 hrs

Item: Image quality in spectroscopic mode using N30 camera
Responsible: LUCI-Team
Phase: AO-Com #2
Procedure: Take spectra with G40-grating, determine spectral and spatial resolution
Weather: Thin cirrus
Prerequisites: Grating G40 implemented
Targets: (Narrow) Emission-line point source (could be QSO @ high-z and/or emisison-line star)
Specs: Results should be same as in lab (spectral resolution) and
as expected from imaging (spatial resolution) (blurring)
Remarks: May also determine effects of diffraction.

Ghosts, Scattered Light, duration 2 hrs

Item: Determination of Ghost intensity, scattered light level in
the instrument in the telescope environment
Responsible: LUCI-Team
Procedure: Imaging with N30 camera, filters and gratings over FOV
Weather: No restrictions
Prerequisites: Bright star without an additional bright star in FOV
Targets: Non-saturated star
Specs: < 5 * 10 * (-3) of incident flux.

Variability of PSF, duration 6hrs

Item: Check variability of an AO corrected star
Responsible: LUCI-Team
Phase: Any phase
Procedure: Take images of stars. Monitor variability of PSF both on short time scales
(several images during one observing run) and on large time scales (during whole
commissioning). Do the same in spectroscopic modes as this will be an important
ingredient for some scientific applications.
Weather: Thin cirrus
Prerequisites:Stars, period(s) of constant seeing (seeing monitor urgently needed)
Targets: Any star which does not saturate, 10-20min time series of DIT=min
Specs: N/A
Remarks: Results will help AO team, data from Strehl-measurements
can be used for variability of PSF on short timescales.

Image movement due to flexure in AO mode, duration 5 hrs

Item: Determine effect of differential flexure between LUCI2
focal plane and AO WFS focal plane in real observing condition.
Responsible: LUCI-Team
Phase: Any phase
Procedure: Determination of PSF displacement on detector when observing
a bright star in closed loop at 8-10 instrument rotator positions and four different elevations.
Weather: Thin cirrus
Prerequisites: A pointing mask equivalent to the one used for SL-com
Targets: Any star.
Specs: 1 pix deviation wrt to peaked value
Remarks: Verification of differential flexure in real observing conditions.

Active flexure compensation, duration 5 hrs

Item: Verify active flexure compensation
Responsible: LUCI-Team
Phase: Com #2
Procedure: Take spectra of point sources in all grating/orders
using faint, intermediate and bright night-sky lines for active flexure
compensation. Determine achievable spectral resolution, optimize time-scales for
correction, verify long-term stability.
Weather: Clear
Targets: Point sources
Specs: Flexure is compensated to +- 0.5 pix in imaging on time-scales of a few minutes
and to +- 1 pix in spectroscopic mode on a timescale of 15 minutes.
Remarks: New, could not be tested during seeing-limited com. May require more time
to be fully implemented and optimized.

-- %USERSIG{JochenHeidt - 2014-12-29}%
Topic revision: r7 - 30 Jan 2015, JochenHeidt
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